Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 401, Issue 1, Pages 405-410Publisher
WILEY-BLACKWELL PUBLISHING, INC
DOI: 10.1111/j.1365-2966.2009.15650.x
Keywords
circumstellar matter; stars: kinematics; stars: mass-loss; stars: winds; outflows; planetary nebulae: individual: SuWt 2; PN G311; 0+02; 4
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Funding
- ANR
- SiNeRGHy [ANR-06-CIS6-009-01]
- Science and Technology Facilities Council [ST/F002270/1, ST/F003196/1] Funding Source: researchfish
- STFC [ST/F003196/1, ST/F002270/1] Funding Source: UKRI
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We present the first detailed spatio-kinematical analysis and modelling of the southern planetary nebula SuWt 2. This object presents a problem for current theories of planetary nebula formation and evolution, as it is not known to contain a central post-main-sequence star. Deep narrow-band [N ii]6584 A images reveal the presence of faint bipolar lobes emanating from the edges of the nebular ring. Long-slit observations of the H alpha and [N ii]6584 A emission lines were obtained using the ESO (European Southern Observatory) Multi-Mode Instrument on the 3.6-m ESO New Technology Telescope. The spectra reveal the nebular morphology as a bright torus encircling the waist of an extended bipolar structure. By deprojection, the inclination of the ring is found to be 68 degrees +/- 2 degrees (cf. similar to 90 degrees for the double A-type binary believed to lie at the centre of the nebula), and the ring expansion velocity is found to be 28 km s-1. Our findings are discussed with relation to possible formation scenarios for SuWt 2. Through comparison of the nebular heliocentric systemic velocity, found here to be -25 +/- 5 km s-1, and the heliocentric systemic velocity of the double A-type binary, we conclude that neither component of the binary could have been the nebular progenitor. However, we are unable to rule out the presence of a third component to the system, which would have been the nebula progenitor.
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